演講資訊

摘要：

Kepler Mission found that earth-sized planets or super-Earths are extremely common around solar-like stars, which has motivated extensive ALMA surveys towards protoplanetary disks to characterize the properties of the dust mass reservoirs for feeding terrestrial planet-formation, and to investigate where and how dust grains grow from (sub)micron sizes to millimeter or larger sizes. Those surveys (e.g., towards the Lupus, Taurus, Ophiuchus molecular clouds, etc.) coherently concluded that the median dust mass is about ten times the Earth-mass, which is barely sufficient for forming those rocky planets observed by Kepler Mission. I will explain the reason why all those previous measurements may have underestimated dust masses by 1-2 orders of magnitude, and have overestimates dust grain sizes by 2-3 orders of magnitude, due to overlooking a subtle radiative transfer effect. I will demonstrate this radiative transfer effect with both 3D radiative transfer modeling and with the actual ALMA observations towards the best resolved protoplanetary disk, TW Hya.